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A&A
Volume 444, Number 1, December II 2005
Page(s) 327 - 336
Section On-line catalogs and data
DOI http://dx.doi.org/10.1051/0004-6361:20052715


A&A 444, 327-336 (2005)
DOI: 10.1051/0004-6361:20052715

Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops

N. Ponthieu1, 2, J. F. Macías-Pérez2, M. Tristram2, P. Ade3, A. Amblard4, R. Ansari5, J. Aumont2, É. Aubourg6, 7, A. Benoît8, J.-Ph. Bernard9, A. Blanchard10, J. J. Bock11, 12, F. R. Bouchet13, A. Bourrachot5, P. Camus8, J.-F. Cardoso14, 7, F. Couchot5, P. de Bernardis15, J. Delabrouille14, 7, F.-X. Désert16, M. Douspis10, L. Dumoulin17, Ph. Filliatre18, P. Fosalba19, M. Giard9, Y. Giraud-Héraud14, 7, R. Gispert1, J. Grain2, L. Guglielmi14, 7, J.-Ch. Hamilton20, S. Hanany21, S. Henrot-Versillé5, J. Kaplan14, 7, G. Lagache1, A. E. Lange12, K. Madet8, B. Maffei3, S. Masi15, F. Mayet2, F. Nati15, G. Patanchon22, O. Perdereau5, S. Plaszczynski5, M. Piat14, 7, S. Prunet13, J.-L. Puget1, C. Renault2, C. Rosset14, 7, D. Santos2, D. Vibert13 and D. Yvon6, 7

1  Institut d'Astrophysique Spatiale, Bât. 121, Université Paris XI, 91405 Orsay Cedex, France
    e-mail: reprints@archeops.org
2  Laboratoire de Physique Subatomique et de Cosmologie, 53 avenue des Martyrs, 38026 Grenoble Cedex, France
    e-mail: macias@in2p3.fr
3  Cardiff University, Physics Department, PO Box 913, 5, The Parade, Cardiff, CF24 3YB, UK
4  University of California, Berkeley, Dept. of Astronomy, 601 Campbell Hall, Berkeley, CA 94720-3411, USA
5  Laboratoire de l'Accélérateur Linéaire, BP 34, Campus Orsay, 91898 Orsay Cedex, France
6  CEA-CE Saclay, DAPNIA, Service de Physique des Particules, Bât 141, 91191 Gif-sur-Yvette Cedex, France
7  Fédération de Recherche APC, Université Paris 7, Paris, France
8  Centre de Recherche sur les Très Basses Températures, BP166, 38042 Grenoble Cedex 9, France
9  Centre d'Étude Spatiale des Rayonnements, BP 4346, 31028 Toulouse Cedex 4, France
10  Laboratoire d'Astrophysique de Tarbes Toulouse, OMP, UPS, CNRS UMR 5572, 14 Av. E. Belin 31400 Toulouse, France
11  California Institute of Technology, 105-24 Caltech, 1201 East California Blvd, Pasadena CA 91125, USA
12  Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California 91109, USA
13  Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
14  Physique Corpusculaire et Cosmologie, Collège de France, 11 Pl. M. Berthelot, 75231 Paris Cedex 5, France
15  Gruppo di Cosmologia Sperimentale, Dipart. di Fisica, Univ. "La Sapienza", P. A. Moro, 2, 00185 Roma, Italy
16  Laboratoire d'Astrophysique, Obs. de Grenoble, BP 53, 38041 Grenoble Cedex 9, France
17  CSNSM-IN2P3, Bât 108, 91405 Orsay Campus, France
18  CEA-CE Saclay, DAPNIA, Service d'Astrophysique, Bât 709, 91191 Gif-sur-Yvette Cedex, France
19  Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr, Honolulu, HI 96822, USA
20  LPNHE, Universités Paris VI et Paris VII, 4 place Jussieu, Tour 33, 75252 Paris Cedex 05, France
21  School of Physics and Astronomy, 116 Church St. S.E., University of Minnesota, Minneapolis MN 55455, USA
22  Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada

(Received 21 January 2005 / Accepted 11 August 2005 )

Abstract
We present the first measurement of temperature and polarization angular power spectra of the diffuse emission of Galactic dust at 353 GHz as seen by Archeops on 20% of the sky. The temperature angular power spectrum is compatible with that provided by the extrapolation to 353 GHz of IRAS and DIRBE maps using Finkbeiner et al. (1999, ApJ, 524, 867) model number 8. For Galactic latitudes $\vert b\vert \geq 5$ deg we report a 4 sigma detection of large scale ( $3\leq \ell \leq 8$) temperature-polarization cross-correlation $(\ell+1)C_\ell^{TE}/2\pi = 76\pm 21\;\mu\rm {K_{RJ}^2}$ and set upper limits to the E and B mode polarization at $11\;\mu\rm {K_{RJ}^2}$. For Galactic latitudes $\vert b\vert \geq 10$ deg, on the same angular scales, we report a 2 sigma detection of temperature-polarization cross-correlation $(\ell+1)C_\ell^{TE}/2\pi = 24\pm 13\;\mu\rm {K_{RJ}^2}$. These results are then extrapolated to 100 GHz to estimate the contamination in CMB measurements by polarized diffuse Galactic dust emission. The TE signal is then $1.7\pm0.5$ and $0.5\pm0.3\;\mu\rm {K^2_{CMB}}$ for $\vert b\vert \geq 5$ and 10 deg respectively. The upper limit on E and B mode polarization becomes $0.2\;\mu\rm {K^2_{CMB}}\;(2\sigma)$. If the physical properties of dust radiation on the fraction of the sky observed by Archeops are representative of the whole sky, and if the actual level of E and B mode polarization is close to this upper limit, then dust polarized radiation will be a major foreground for determining the polarization power spectra of the CMB at high frequencies above 100 GHz.


Key words: cosmology: cosmic microwave background -- cosmology: observations -- polarization -- ISM: dust, extinction

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